I still stand by my post. Gravity is found in everything and has a value.
Mass is determined by size of a planet. This can be seen with the moon landings. Smaller than Earth.
So if the so called Black hole is in fact a massive planet with such massive gravity that light can not escape it would look like a hole. At some point the gravity gets so great it changes the planet as you all know.
Actually gravity does not explain the observed movements observed in the universe and as far as black holes are concerned nothing is known only speculated. Bye the way a hole in space would not look any different than the empty space around it also please explain how a lightless hole can have size. The thing everyone misses is that the radiation coming out of or surrounding the hole is that this would be in the form of a 3d shell surrounding the hole and hiding the entire thing making photography impossible, theoretically anyway
But you use big letters to detail why you failed algebra
Anything with a large gravitational mass would accelerate things towards it, with greater velocity as they come near. But nothing is going to be going straight at the black hole because the black hole also has a velocity, and in effect is moving out of the way. So the result of that is an accretion disk.
{... An
accretion disk is a structure (often a
circumstellar disk) formed by diffuse material in
orbital motion around a massive
central body. The central body is typically a
star.
Friction causes orbiting material in the disk to spiral inward towards the central body. Gravitational and frictional forces compress and raise the temperature of the material, causing the emission of
electromagnetic radiation. The frequency range of that radiation depends on the central object's mass. Accretion disks of young stars and
protostars radiate in the
infrared; those around
neutron stars and
black holes in the
X-ray part of the
spectrum. The study of oscillation modes in accretion disks is referred to as
diskoseismology
...
Accretion disks are a ubiquitous phenomenon in astrophysics; active galactic nuclei, protoplanetary disks, and gamma ray bursts all involve accretion disks. These disks very often give rise to astrophysical jets coming from the vicinity of the central object. Jets are an efficient way for the star-disk system to shed angular momentum without losing too much mass.
The most spectacular accretion disks found in nature are those of active galactic nuclei and of quasars, which are thought to be massive black holes at the center of galaxies. As matter enters the accretion disc, it follows a trajectory called a tendex line, which describes an inward spiral. This is because particles rub and bounce against each other in a turbulent flow, causing frictional heating which radiates energy away, reducing the particles' angular momentum, allowing the particle to drift inwards, driving the inward spiral. The loss of angular momentum manifests as a reduction in velocity; at a slower velocity, the particle wants to adopt a lower orbit. As the particle falls to this lower orbit, a portion of its gravitational potential energy is converted to increased velocity and the particle gains speed. Thus, the particle has lost energy even though it is now travelling faster than before; however, it has lost angular momentum. As a particle orbits closer and closer, its velocity increases, as velocity increases frictional heating increases as more and more of the particle's potential energy (relative to the black hole) is radiated away; the accretion disk of a black hole is hot enough to emit X-rays just outside the event horizon. The large luminosity of quasars is believed to be a result of gas being accreted by supermassive black holes.[3] Elliptical accretion disks formed at tidal disruption of stars can be typical in galactic nuclei and quasars.[4] Accretion process can convert about 10 percent to over 40 percent of the mass of an object into energy as compared to around 0.7 percent for nuclear fusion processes.[5] In close binary systems the more massive primary component evolves faster and has already become a white dwarf, a neutron star, or a black hole, when the less massive companion reaches the giant state and exceeds its Roche lobe. A gas flow then develops from the companion star to the primary. Angular momentum conservation prevents a straight flow from one star to the other and an accretion disk forms instead.
...}
Accretion disk - Wikipedia